A catalogue of ionized gas velocity fields for a sample of 30 spiral and irregular galaxies of the Virgo cluster has been obtained by using 3D optical data. The aim of this survey is to study the influence of high-density environments on the gaseous kinematics of local cluster galaxies. Observations of the Hα line by means of Fabry-Perot interferometry have been performed at the Canada-France-Hawaii Telescope, European Southern Observatory 3.6-m telescope, Observatoire de Haute-Provence 1.93-m telescope and Observatoire du mont Mégantic telescope at angular and spectral samplings from 0.4 to 1.6 arcsec and 7 to 16 km s −1 . A recently developed, automatic and adaptive spatial binning technique is used to reach a nearly constant signal-to-noise ratio (S/N) over the whole field of view, allowing us to keep a high spatial resolution in high-S/N regions and extend the detection of signal in low-S/N regions. This paper is part of a series and presents the integrated emission-line and velocity maps of the galaxies. Both Hα morphologies and kinematics exhibit signs of perturbations in the form of, for example, external filaments, inner and nuclear spiral-and ring-like structures, inner kinematical twists, kinematical decoupling of a nuclear spiral, streaming motions along spiral arms and misalignment between kinematical and photometric orientation axes.

Abstract. GHASP (Gassendi Hα survey of SPirals) is a survey of Hα velocities in spiral and irregular galaxies. The observations began in 1998, with a scanning Fabry-Perot and a focal reducer attached at the Cassegrain focus of the 1.93 m telescope at the Observatoire de Haute-Provence. This paper presents the Hα maps, the 2D velocity fields and the rotation curves obtained for a set of 23 galaxies observed in October 1998 and April 1999. Most of them have already been observed in HI in the frame of the WHISP survey led at Westerbork, for which GHASP brings an interesting complement. The aim is to provide a reference sample of 2D velocity fields for about 200 nearby spiral galaxies at Hα wavelength.

Abstract. We present Fabry Perot observations of galaxies in five Hickson Compact Groups: HCG 10, HCG 19, HCG 87, HCG 91 and HCG 96. We observed a total of 15 galaxies and we have detected ionized gas for 13 of them. We were able to derive 2D velocity, monochromatic, continuum maps and rotation curves for the 13 objects. Almost all galaxies in this study are late-type systems; only HCG 19a is an elliptical galaxy. We can see a trend of kinematic evolution within a group and among different groups -from strongly interacting systems to galaxies with no signs of interaction -HCG 10 exhibits at least one galaxy strongly disturbed; HCG 19 seems to be quite evolved; HCG 87 does not show any sign of merging but a possible gas exchange between two galaxies; HCG 91 could be accreting a new intruder; HCG 96 exhibits past and present interactions.

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We report on kinematic observations of Ha emission from four late-type galaxies of Hickson Compact Group 16 (H16a, b, c, d) obtained with a scanning Fabry-Perot interferometer and samplings of 16 km s~1 and 1A. The velocity Ðelds show kinematic peculiarities for three of the four galaxies : H16b, H16c, and H16d. Misalignments between the kinematic and photometric axes of gas and stellar components (H16bÈH16d), double gas systems (H16c) and severe warping of the kinematic major axis (H16b and H16c) were some of the peculiarities detected.We conclude that major merger events have taken place in at least two of the galaxies of the group, H16c and H16d, based on their signiÐcant kinematic peculiarities, their double nuclei, and their high infrared luminosities. Their Ha gas content is strongly spatially concentrated ; H16d contains a peculiar barlike structure conÐned to the inner D1 h~1 kpc region. These observations are in agreement with predictions of simulations, namely, that the gas Ñows toward the galaxy nucleus during mergers, forms bars, and fuels the central activity. Galaxy H16b, an Sb galaxy, also presents some of the kinematic evidence for past accretion events. Its gas content, however, is very sparse, limiting our ability to Ðnd other kinematic merging indicators, if they are present. We Ðnd that the merger remnants in the compact group HCG 16 have signiÐcantly smoother optical proÐles than isolated mergers, i.e., they show an amorphous morphology and no signs of tidal tails. Tidal arms and tails formed during the mergers may have been stripped by the group potential, or, alternatively, they may have never been formed.The velocity Ðeld of the galaxy H16a shows grand-design isovelocity lines with no signs of disturbances inside a radius of This result is contrary to expectations given that the galaxy has a DR 25 . high infrared luminosity, central activity, tidal tails at large radii, and is embedded in a common group envelope observed in H I and X-rays. The normality of the velocity Ðeld suggests that this galaxy may be a fairly recent acquisition of the compact group.Our observations suggest that HCG 16 may be a young compact group in formation through the merging of close-by objects in a dense environment.